r-Mode in Young Neutron Stars
[Drawn from Lindblom, Tohline & Vallisneri (2001, 2002)]
Simulation Technique
Governing Equations for CFD Simulations
Explicit Time-Integration
Finite-Difference Scheme
Uniform, Cylindrical Lattice
(no AMR)
[ Typically (128,256,90) in (R,
q
,Z) ]
Rotating Frame
van Leer Advection
[
a la
ZEUS-2D
]
Heterogeneous Computing Environment
CACR: HP Exemplar
Initial Equilibrium Configuration
HSCF technique
Uniformly rotating, n = 1 Polytrope
(E
_{rot}
/|E
_{grav}
| = 0.10)
Perturb model with
linearized r-mode velocity field
Simulation Results
M = 1.4 solar masses
R
_{0}
= 12.5 km (R
_{eq}
= 18.4 km)
P = 1.18 ms
Radiation Reaction Force artificially enhanced by factor of
4500
("c" reduced by factor of 3.32)
Development of eigenfunction
during linear-amplitude regime.
Evolution at nonlinear amplitude
Title Page